text:
\section{Introduction}
\label{intro}

The correlations of black hole mass with galaxy properties
imply a close link between black hole growth and galaxy evolution
\citep{FM00, Gt00, gultekin+09, woo10}.
Numerous theoretical and observational studies have been dedicated
to revealing the nature of the connection
(e.g., Kauffmann \& Haehnelt 2000; Springel et al. 2005;
Croton et al. 2006; Woo et al. 2006, 2008; Hopkins et al. 2007;
Merloni et al. 2010; Bennert et al. 2011).

Probing the direct connection between starburst and
active galactic nuclei (AGN) can shed light on how black hole
growth and bulge growth are inter-connected.
However, it is challenging to observationally measure both the starburst rate
and AGN activity for given galaxies.
Optically-identified broad-line AGNs are the best objects for measuring
black hole mass and AGN accretion rate. On the other hand the star formation rate of
host galaxies is difficult to measure
since AGN flux dominates in the UV continuum and hydrogen recombination lines,
i.e., H$\alpha$, which are generally used as a star formation indicator
in non-AGN galaxies.
In the case of Type II AGN, it is relatively easy to measure star formation
rate while black hole mass and accretion rate are difficult to determine
owing to the dust obscuration of accretion disk and broad-line region.

The polycyclic aromatic hydrocarbon (PAH) emission features emitted by small
carbon grains are one of the star formation indicators.
Thus, PAH emissions have been used to constrain star formation
activity in the host galaxies of Type 1 AGN (e.g., Ogle et al. 2006; Schweitzer et al. 2006;
Shi et al. 2007).
Based on the ground-based and space observations, various PAH emission features,
i.e., 3.3, 6.2, 7.7, 8.6, 11.3, and 12.7 $\mu m$~lines,
have been detected in many local Seyfert 1 galaxies and distant QSOs
although not all AGN show PAH emission features
\citep[e.g.,][]
{clavel+00, Rod03, imanishi04, ntz07,lz07,lutz+08,shi+09,imanishi10,Oi10,imanishi11}.

Among PAH-detected AGN, there seems to be a correlation between
nuclear starburst and AGN activity. Using
a sample of low-redshift Palomar-Green (PG) QSOs observed with
the Spitzer Infrared Spectrograph (IRS), \citet{ntz07}
showed that 7.7 $\mu m$~PAH luminosity increases
with AGN continuum luminosity at 5100\AA~ (L$_{\rm 5100\AA}$), indicating the starburst-AGN connection.
High-redshift QSOs seem to follow the same trend, extending the correlation
to much higher luminosity range \citep{lutz+08}.
The starburst-AGN connection is supported by a number of theoretical studies,
demonstrating that both nuclear starburst events
and AGN activity
can be triggered by gas inflow through galaxy interactions
(e.g., Kauffmann \& Haehnelt 2000; Robertson et al. 2006;
Ciotti \& Ostriker 2007; Hopkins et al. 2009).

For lower luminosity AGNs it is less clear how AGN activity
is connected to starburst since AGN power is more difficult to measure
owing to increasing host galaxy contribution in lower luminosity AGN.
Based on the ground-based L-band slit spectra,
\citet{imanishi04} measured the 3.3 $\mu m$~PAH luminosity of local Seyfert 1 and 2 galaxies,
showing a positive correlation between starburst and
AGN activity although the correlation is not tight with a large scatter.
In their study, radio luminosity and N-band luminosity within 1.5''
of the host galaxies are used as an indicator of AGN power.
Using 2-10 kev X-ray luminosity, \citet{Wt08} showed a similar trend
between AGN power and the 3.3 $\mu m$~PAH luminosity for a larger sample
of local Seyfert 1 and 2 galaxies.

Most previous observational studies on PAH features with ground based
long-slit spectroscopy or Spitzer IRS observations have probed the
inner part of galaxies, indicating a connection between {\it nuclear} starburst within a few kpc
and AGN activity \citep[e.g.,][]{Wt08}.
In contrast, whether global star formation over
entire galaxies is related with AGN activity it is not well studied
since most previous studies, particularly for local and low-redshift galaxies,
have used a relatively small aperture to extract PAH emission features,
measuring nuclear PAH emissions.
Based on the spatially resolved mid-IR spectroscopy of nearby active galaxies,
several studies have reported that
PAH emissions are mainly from the disk \citep[e.g.,][]{laurent+00, lefloch+01},
suggesting that the global PAH luminosity measured over entire galaxies
may be much larger than nuclear PAH luminosity.

In this paper, we investigate global and nuclear star formation in the
host galaxies of Type 1 AGN, using the 3.3 $\mu m$~PAH emission measurements
based on our new observations with the AKARI space telescope and
collected data from the literature.
The AKARI telescope provides a unique capability of slit-less spectroscopy
to measure global star formation over entire galaxies
(e.g., Imanishi et al. 2010).
This paper is organized as follows. In \S \ref{data}, we describe
sample selection,
observations and data reduction of the AKARI observations.
We present 3.3 $\mu m$~PAH emission measurements in \S \ref{analysis}.
Main results on the starburst-AGN connection are presented in \S \ref{results}.
Discussion and conclusions are followed in \S~5.
Throughout the paper, we assume a Hubble constant of
H$_{o}$ = 70 km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\Lambda} =0.7$, and $\Omega_{M} = 0.3$.

\section{Observations and Data Reduction}
\label{data}

\subsection{Sample Selection}
\label{sample}

We selected a sample of 27 moderate-luminosity AGN (L$_{\rm 5100\AA}$ $\sim$ 0.1-3 $\times$
10$^{44}$ erg s$^{-1}$) at 0.35 $<$ z $<$ 0.36 from the Sloan Digital
Sky Survey Data Release 7 to study star formation activity based on the PAH feature
at 3.3 $\mu m$. The sample was initially selected for investigating the evolution
of the black hole mass-stellar velocity dispersion (M$_{\rm BH}-\sigma_{*}$) relation. Details of sample selection can be found in \citet{woo06} and \citet{treu07}.
In summary, we selected broad-line AGNs with the H$\beta$ equivalent width (EW) $>$ 5 \AA~
to properly estimate black hole masses based on the kinematics of broad-line region gas.
The specific redshift range was selected to avoid
sky emission lines on the stellar absorption features, from which stellar velocity dispersions
were directly measured.
The spectral energy distribution of 24 objects in the sample was in detail investigated
by \citep{szathmary11}
based on the multi-wavelength data including Chandra X-ray observations, HST imaging,
and Spitzer IRAC and MIPS imaging as well as the archival data of GALEX and
Two Micron All-Sky Survey (2MASS).
From the spectral energy distribution (SED) fitting analysis,
AGN SED was separated from galaxy SED,
leading to accurate measurements of AGN bolometric luminosities.
Black hole mass of each AGN was estimated by the single-epoch virial method,
which combines the line width of H$\beta$~and the optical luminosity at 5100\AA (L$_{5100}$),
utilizing the size-luminosity relation of the reverberation sample (Bentz et al.
2009) and the most recent calibration of the virial factor by \citet{woo10} (see Table 1).
The black hole mass of the sample covers an order of magnitude, i.e., $7.6 < \log$ M$_{\rm BH}$/M$_{\odot}$ $< 8.7$.
Combining black hole mass estimates with the bolometric luminosities measured
from the SED fitting, we obtained the Eddington ratios, ranging from  a few to $\sim$50\%
of the Eddington limit. The basic properties of the sample are listed in Table \ref{table1}.

\begin{deluxetable*}{cccccccccc}
\tabletypesize{\scriptsize}
\tablecaption{Properties of the AKARI sample: Type I AGN at z$\sim$0.4
\label{table1}
}
\tablewidth{0pt}
\tablehead{
\colhead{Name}
&\colhead{RA (J2000)} &\colhead{DEC (J2000)}
&\colhead{redshift}
&\colhead{log L$_{bol}$}
&\colhead{$\lambda$L$_{5100,nuc}$}
&\colhead{$f_{nuc}$}
&\colhead{log L$_{X}$}
&\colhead{log M$_{\rm BH}$}
&\colhead{pointings} \\
\colhead{}
&\colhead{} &\colhead{}
&\colhead{}
&\colhead{(erg/s)}
&\colhead{(erg/s)}
&\colhead{}
&\colhead{(erg/s)}
&\colhead{(M$_{\odot}$)}
&\colhead{}    \\
\colhead{(1)}  &
\colhead{(2)}  &
\colhead{(3)}  &
\colhead{(4)}  &
\colhead{(5)}  &
\colhead{(6)}  &
\colhead{(7)}  &
\colhead{(8)}  &
\colhead{(9)}  &
\colhead{(10)} \\
}
\startdata

S01	& 15 39 16.23 & +03 23 22.1 & 0.3592	& 45.23 & 0.72 & 0.29 & 44.48 & 8.20 	 &1\\
S02	& 16 11 11.67 & +51 31 31.1 & 0.3544	& 45.13 & 0.34 & 0.22 &	44.60 & 7.98  &  4	\\
 S03	& 17 32 03.11 & +61 17 52.0  & 0.3583	& 45.50 & 1.64 & 0.39 & 44.95 & 8.28  & 4\\
 S04	& 21 02 11.51 & -06 46 45.0 & 0.3578	& 45.27 & 1.33 & 0.36 &	44.55 & 8.44  &4 \\
 S05	& 21 04 51.85 & -07 12 09.4 & 0.3530  	& 45.44 & 1.85 & 0.47 & 44.84 & 8.74 &4\\
 S06	& 21 20 34.19 & -06 41 22.2 & 0.3684  	& 45.05 & 0.51 & 0.18 &	44.25 & 8.16 &4\\
 S07	& 23 09 46.14 & +00 00 48.9 & 0.3518  	& 45.47 & 2.10 & 0.45 &	44.80 & 8.53  &2\\
 S08	& 23 59 53.44 & -09 36 55.5 & 0.3585	& 45.23 & 1.22 & 0.40 & 44.55 & 8.10    &4\\
 S09	& 00 59 16.11 & +15 38 16.1  & 0.3542	& 45.37 & 0.71 & 0.22 & 44.78 & 8.13  &4\\
S10	& 01 01 12.07 & -09 45 00.8  & 0.3506	& 45.48 & 1.02 & 0.27 & 44.93 & 8.25 &4\\
 S11	& 01 07 15.97 & -08 34 29.4 & 0.3557	& 45.34 & 0.52 & 0.14 & 44.85 & 8.00	  &4\\
 S12	& 02 13 40.60 & +13 47 43.3  & 0.3570	& 45.43 & 0.97 & 0.28 & 44.62 & 8.67	  &4\\
 S21	& 11 05 56.18 & +03 12 43.3  & 0.3534  	& 45.88 & 2.15 & 0.34 &	44.06 & 8.79   &1\\
 S23	& 14 00 16.66 & -01 08 22.2  & 0.3510  	& 45.42 & 1.11 & 0.29 & 44.75 & 8.70  &3\\

 S26	& 15 29 22.26 & +59 28 54.6  & 0.3691	& 45.13 & 0.52 & 0.27 & 44.38 & 8.02	   &4\\
 S27	& 15 36 51.28 & +54 14 42.7 & 0.3667	& 45.23 & 0.95 & 0.36 & 44.74 & 8.10  &4\\
 S28	& 16 11 56.30 & +45 16 11.0 & 0.3680  	& 45.13 & 0.76 & 0.03 & 44.66 & 7.90  &4\\
 S29	& 21 58 41.93 & -01 15 00.3 & 0.3575  	& 45.43 & 0.59 & 0.10 & 44.54 &	7.94  &4\\
 S31	& 10 15 27.26 & +62 59 11.5 & 0.3504	& 45.38 & 0.29 & 0.08 & 44.58 & 7.94  &2\\
 SS1	& 08 04 27.99 & +52 23 06.2 &	0.3566	& 45.41 & 0.39 & 0.11 & 44.89 & 7.75	 &4\\
 SS2	& 09 34 55.60 & +05 14 09.1 & 	0.3675	& 45.21 & 0.33 & 0.13 & 44.54 & 7.72  & 	3\\
 SS9	& 12 58 38.71 & +45 55 15.5 & 0.3704	& 44.92$^a$ & 0.93 &0.26& \nodata & 8.05	&4\\
 SS10   & 13 34 14.84 & +11 42 21.5 & 0.3658	& 45.30$^a$ & 2.26 &0.43& \nodata & 7.94   &4\\
 SS11   & 13 52 26.90 & +39 24 26.8 & 0.3732	& 44.66$^a$ & 0.51 &0.15& \nodata & 8.11 &4\\
 SS12   & 15 01 16.83 & +53 31 02.4 & 0.3626	& 45.46$^a$ & 3.24 &0.52& \nodata & 8.15 &4\\
 SS13   & 15 05 41.79 & +49 35 20.0 & 0.3745    & 44.94$^a$ & 0.98 &0.38& \nodata & 7.63  &4
\enddata

\tablecomments{
Col. (1): Object name.
Col. (2): RA.
Col. (3): DEC.
Col. (4): redshift
Col. (5): AGN bolometric luminosity measured from multi-wavelength data,
adopted from \citet{szathmary11}.
Col. (6): AGN monochromatic luminosity at 5100\AA~ in 10$^{44}$ erg s$^{-1}$~ units,
corrected for host galaxy starlight based on the HST images,
taken from \citet{treu07, bennert10}.
Col. (7): AGN fraction in the observed flux at 5100\AA, adopted from
\citet{treu07, bennert10}.
Col. (8): AGN X-ray luminosity from \citet{szathmary11}.
Col. (9): Black hole mass estimated from H$\beta$~line width and L$_{5100}$
adopted from \citet{woo06,bennert10}.
Col. (10): Number of pointings for AKARI observation
}

\tablenotetext{a}{AGN bolometric luminosity is calculated from
optical luminosity (L$_{5100}$) assuming that
L$_{bol}$ = 9 $\times \lambda$ L$_{5100}$.}

\end{deluxetable*}

\subsection{AKARI Observations}
\label{obs}

To detect the PAH features at the rest-frame $\sim$3.3 $\mu m$, we carried out spectroscopic
observations using the Infrared Camera (IRC) on board the AKARI space telescope
\citep{IRC}. The field of view of IRC is roughly 10' $\times$ 10' with
a spatial scale of 1.45''/pixel.
The full-width-at-half-maximum of the point spread function is 3.2 pixels,
corresponding to 4.64''.
The NIR grism mode (NG) was adopted for most of the observations,
providing spectral resolution of R $\sim$ 120 at 3.6 $\mu m$~ for a point source \citep{IRC}.
A unique capability of IRC is the slit-less spectroscopic mode.
With 1' by 1' aperture used for pointing mode, the photons from the
entire galaxies in our sample can be detected.
Thus, the measured 3.3 $\mu m$~PAH luminosities represent
the {\it global} star formation.

The exposure time for each AGN host galaxy was determined in order to
achieve signal-to-noise ratio S/N $>$ 10 in the continuum.
We assigned 4 pointings (6 minute exposure per pointing) for each target
based on the exposure time calculation using the K-band magnitudes
from the 2MASS archive.
Owing to the complexity of scheduling of the sun-synchronous
polar orbit of the AKARI, a couple of objects were observed with less than 4 points.
In summary, we obtained a total of 93 pointings for 27 target galaxies
(see \ref{table1}).

\subsection{Data Reduction}
\label{dr}

We carried out data reduction using the IRC spectroscopy pipeline\footnote{ http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/DataReduction/IRC/}.
The data reduction procedures with the IRC spectroscopy pipeline
is described in detail by \citet{IRCpipe}.
In summary, the reduction steps include standard procedures:
dark subtraction, linearity correction, flat-fielding,
background subtraction, extraction of 2-dimensional spectra,
wavelength calibration, and flux calibration.
Before extracting 1-dimensional spectra,
we applied additional cosmic ray removal using {\it L.A.Cosmic} \citep{laC}
to remove hot pixels, which significantly increased in Phase 3 (post liquid-He warm
mission cooled by the onboard cryocooler).
To extract 1-dimensional spectra, we used five pixels along the spatial
direction as recommended by \citet{IRCpipe}.
As a consistency check, we compared the spectra extracted from
larger aperture sizes and found no difference in the extracted spectra.
Finally, we combine the extracted 1-dimensional spectra from each pointing
while applying additional sigma-clipping.
In order to improve signal-to-noise ratio, we apply three pixels binning
along the wavelength direction.
We were not able to extract a spectrum for one object (S10) due to the low
quality of the observed spectral images. Thus, this target is excluded
for the following analysis.

\begin{figure}
\begin{center}
\includegraphics[scale=0.5]{f1.eps}
\caption{AKARI spectra of moderate-luminosity AGN at z$\sim$0.4 with the 3.3 $\mu m$~PAH emission detection. The location of the 3.3 $\mu m$~PAH emission is indicated by an arrow in each
panel.
\label{fig1}}
\end{center}
\end{figure}

\section{3.3 $\mu m$~PAH measurements}
\label{analysis}

\subsection{Individual galaxies}
\label{indiv}

In Figure \ref{fig1} we present the reduced spectra of 7 galaxies
with the 3.3 $\mu m$~PAH emission detection.
Due to the low signal-to-noise ratio of the observed spectra,
it is necessary to assume an intrinsic profile of the 3.3 $\mu m$~PAH emission line
in order to confirm the detection of the line and measure its strength.
In measuring the line strength of the PAH emission lines,
several different fitting schemes with various line profiles,
i.g., Gaussian, Lorentzian, Drude profiles, and Spline functions have been devised.
For example, \citet{Ga08} applied Spline functions and Lorentz profiles
for fitting PAH emission lines in various sources and found no
systematic difference in the measured PAH fluxes while
\citet{Sm07} applied Drude profile to mid-IR
spectra obtained from the $Spitzer$ IRS.
We chose a Gaussian profile, which is generally adopted for
the 3.3 $\mu m$~PAH emission lines observed in starburst galaxies
(Type-A sources in Tokunaga et al. 1991).
In practice, we applied a Gaussian profile with a fixed width
in the rest-frame for modeling the 3.3 $\mu m$~PAH line.
We adopted 21 nm as a fixed width of the line profile, which has been
determined from the PAH line profile of M82 (Tokunaga et al. 1991) and
used for our previous studies of the 3.3$\mu m$~PAH line based on
the AKARI IRC spectra (Imanishi et al. 2008, 2010).

Continuum subtraction is the largest source of uncertainty in measuring PAH
emission line flux since absorption features are abundant in the near- and mid-IR
spectral ranges. The vicinity of the 3.3 $\mu m$ PAH feature
is not an exception: There is a plethora of absorption features in the rest-frame
2 - 5 $\mu m$~range.
We applied a linear fit to the continuum in the 3.0 - 3.6 $\mu m$~range
with two-pixel binning,
after masking the location of the PAH feature around the 3.3 $\mu m$,
as similarly practiced in other studies \citep[e.g.][]{imanishi04,imanishi10,Oi10,imanishi11}.

While fitting the 3.3 $\mu m$ PAH feature by a Gaussian profile,
we determined the peak and the central wavelength of the profile
based on the $\chi^2$ minimization. Then, the line flux and the equivalent width
were determined from the fit (see Table \ref{table2}).
The typical error of the measured flux density is $\sim 3 \times 10^{-14}$ erg s$^{-1}$ cm$^{-2}$ $$\mu m$^{-1}$.

We detected the 3.3 $\mu m$~PAH feature from 7  out of 26
observed galaxies, resulting in a detection rate of 27\%.
Compared to higher luminosity AGN, the 3.3 $\mu m$~PAH detection rate of
our lower-luminosity AGN is slightly higher although the difference
is not easy to interpret owing to the different exposure time and flux limits.
For example, \citet{imanishi11}
investigated the PAH emission features of 30 PG QSOs based on the ground-based
observations, and detected the 3.3$\mu m$~PAH emission from 5 QSOs,
resulting in a $\sim$ 17\% detection rate.
If we exclude S3 and SS12, for which 3.3$\mu m$~PAH emission is marginally
detected, then the detection rate of our lower-luminosity AGN decreases
to 19\%, suggesting that the detection rate is similar to that of PG QSOs.

Compared to the detection rate of other PAH lines at longer wavelength
(e.g., 6.7, 7.7, 8.6, 11.2 $\mu m$) in local Seyfert galaxies,
the detection rate of the 3.3$\mu m$~PAH line in our sample seems to be much lower
(see Sales et al. 2010). This difference may be due to the fact that
3.3$\mu m$~PAH is much weaker than other lines at longer wavelength,
thus more difficult to be detected.
For better understanding of the relation among various PAH lines,
spectroscopic studies with a large spectral range including 3.3$\mu m$~and
other PAH lines are required.

The detected 3.3 $\mu m$~PAH line luminosity (L$_{\rm 3.3~PAH}$) ranges from $\sim 0.9-5.7 \times 10^{42}$
erg s$^{-1}$~ while the upper limit of the PAH luminosity of the undetected galaxies
is close to $\sim 10^{42}$ erg s$^{-1}$.
Compared to the 3.3 $\mu m$~PAH luminosity range
of Type I AGN host galaxies measured from ground-based observations
(L$_{\rm 3.3~PAH}$=10$^{39}$ - 10$^{42}$ erg s$^{-1}$),
the 3.3 $\mu m$~PAH luminosities from the AKARI slit-less spectroscopy are more
than a factor of 10 higher. This is probably due to the aperture effect,
reflecting the difference between nuclear and global star formation.
Ground-based observations generally used a narrow-slit to probe nuclear starburst
while AKARI slit-less spectroscopy provides the global star formation
rate over entire galaxies. A direct comparison between ground-based
and AKARI observations supports this interpretation. For example,
a recent AKARI study by \citet{imanishi10} reported the 3.3 $\mu m$~PAH
luminosity of NGC 7469 as $6.3\times 10^{41}$ erg s$^{-1}$~ while the ground-based
spectroscopy with a 1.6'' slit width by \citet{imanishi04} presented
an upper limit of $2.7\times 10^{40}$erg s$^{-1}$, indicating that the nuclear
PAH emission is a small fraction of the global PAH emission.

For galaxies with no 3.3 $\mu m$ PAH emission detection, we measured the upper limits.
First, we averaged the 1 $\sigma$ errors at the wavelength range of the
expected 3.3 $\mu m$~PAH line. Then, we assumed a Gaussian profile with a peak
flux, which is 3 times larger than the average 1 $\sigma$ error.
In the case of the line width of the profile,
we used a constant width of 21 nm in the rest-frame.
The measurements and upper limits of the 3.3 $\mu m$~PAH luminosity are listed
in Table 2.

\subsection{Combined Spectra}
\label{stack}

In order to construct the representative spectra of the sample
and to recover the undetected 3.3 $\mu m$~PAH in individual galaxies,
we constructed two combined spectra respectively for the entire sample and the galaxies
with no 3.3 $\mu m$~PAH emission detection.
To construct stacked spectra, we used a wavelength range between 3.1 - 3.5 $\mu m$~
in the rest frame and normalized individual spectra by a continuum fit.
Then, we summed individual spectra without weighting.
We also applied two-pixel binning to the data points outside of the 3.3 $\mu m$~PAH line
to smooth the continuum.
The stacked spectra of the entire sample and the galaxies with no 3.3 $\mu m$~PAH detection
are presented in Figure \ref{fig2}.

The combined spectrum of the entire sample clearly shows the 3.3 $\mu m$ PAH emission.
By fitting the PAH emission using a Gaussian profile with a width of 21 nm,
we measured the EW of the 3.3 $\mu m$ PAH line.
The EW of PAH in our sample is larger than that of QSOs. For example,
based on a sample of PG QSOs, \citet{imanishi11} reported that
the EWs of the 3.3 $\mu m$~PAH emission of individual galaxies are typically less than 10 nm
while the EW of the 3.3 $\mu m$~PAH emission measured from their combined spectrum is only 1 nm.
The smaller EW of PAH emission in higher luminosity AGN may be
interpreted to mean that PAH lines are diluted by higher AGN continuum.
However, a larger sample is required to reveal the origin of the trend.

\begin{figure}
\begin{center}
\includegraphics[angle=90, scale=0.4]{f2.eps}
\caption{Stacked spectra of the AKARI sample. The upper panel shows the spectrum stacked with the entire sample of 26 galaxies, while the bottom panel shows the spectrum spectrum stacked with the galaxies without the 3.3 $\mu m$~PAH emission detected. These stacked spectra are the sum of normalized individual spectra within the wavelength range of 3.1 to 3.5 $\mu m$~in the rest frame. We also apply two pixel binning to the data points outside the 3.3 $\mu m$~PAH emission feature.
\label{fig2}}
\end{center}
\end{figure}

\begin{deluxetable}{cccc}
\tablecaption{Global 3.3 $\mu m$~PAH emission measurements based on the AKARI observations
\label{table2} }
\tablewidth{0pt}
\tablehead{
\colhead{Object}
&\colhead{f$_{3.3 \mu m}$}
&\colhead{L$_{3.3 \mu m}$}
&\colhead{EW$_{3.3 \mu m}$}  \\
\colhead{}
&\colhead{(10$^{-15}$ erg s$^{-1}$ cm$^{-2}$)}
&\colhead{(10$^{42}$ erg s$^{-1}$)}
&\colhead{(nm)}   \\
\colhead{(1)}  &
\colhead{(2)}  &
\colhead{(3)}  &
\colhead{(4)}  \\
}

\startdata
 S01	 & < 5.09  & <2.19  & ....\\
 S02	 & < 10.47 & <4.36 & .... \\
 S03	 & 3.10    & 1.33  & 9\\
 S04	 & < 1.55& <0.66  & .... \\
 S05	 & < 2.00& <0.83  & .... \\
 S06	 &< 2.03& <0.93  & .... \\
 S07	 &< 2.76 & <1.13  & .... \\
 S08	 & 3.80    & 1.63  & 87 \\
 S09     & < 31.41 & < 13.07 & .... \\
S10	& .... & .... & .... \\
 S11	&4.40& 1.85  & 21\\
 S12     & < 1.77  & < 0.75 & .... \\
 S21	 & < 12.73 & <5.27  & .... \\
 S23	 &<  1.97 &<0.80 & .... \\
 S26	 & 12.50 &5.73  & 206 \\
 S27	 & < 1.69  &<0.76 & .... \\
 S28	 &6.65 & 3.03  &43 \\
 S29	 & < 1.51 & <0.64 & .... \\
 S31	 & < 1.43  & <0.58 & .... \\
 SS1	 & < 1.77  & <0.74 & .... \\
 SS2	 & < 1.84  & <0.83 & .... \\
 SS3 & < 1.57 &<0.66 & .... \\
 SS9 & < 1.72 &<0.79 & .... \\
 SS10  & < 1.56 &<0.70 & .... \\
 SS11 &  7.15 &3.36 & 77\\
 SS12 & 2.00 &0.88  & 3 \\
 SS13 & < 1.74 	& <0.82 & .... \\
 Stacked & & & 21
\enddata

\tablecomments{Col. (1): Object name. Col. (2): 3.3 $\mu m$~PAH line flux. Col. (3). 3.3 $\mu m$~PAH line luminosity.
Col. (4). Equivalent width of the 3.3 $\mu m$~PAH emission line.
}
\end{deluxetable}

\begin{figure}
\epsscale{1.2}
\plotone{f3.eps}
\caption{Comparison of the 3.3$\mu m$~PAH luminosity (L$_{\rm 3.3~PAH}$) with
the observed total luminosity at the rest-frame 5100 $\AA$ (L$_{\rm 5100\AA}$) ({\it left})
and AGN luminosity corrected for host galaxy starlight contribution ({\it right}).
Filled circles represent the PAH detected galaxies while open circles represent
upper limits of L$_{\rm 3.3~PAH}$. Note that the monochromatic luminosity at 5100\AA~
includes the contribution from
starlight, which is substantial fraction of the total flux (74\% on average).
\label{fig3}}
\end{figure}

\section{Starburst-AGN Connection}
\label{results}

In this section, we investigate how starburst and AGN activity
is related. First, we compare AGN activity with the global star formation
rate measured from the AKARI observations (\S~4.1).
Then, we investigate the correlation between nuclear starburst and
AGN activity based on the collected data from the literature (\S~4.2).

\subsection{Global PAH emission and AGN activity}
\label{Global}

To investigate the relation between global star formation and AGN activity,
we compare the luminosity of the 3.3 $\mu m$~PAH emission (L$_{\rm 3.3~PAH}$) with various
AGN properties, i.e., optical, X-ray, and bolometric luminosities.
First, in Figure 3 (left) we compare the L$_{\rm 3.3~PAH}$~with AGN continuum luminosity
at 5100\AA~(L$_{\rm 5100\AA}$) measured from high S/N optical spectra
obtained with the Low Resolution Imaging Spectrograph at the Keck Telescope \citep{woo06,bennert10}.
Although the optical luminosity range is rather limited, we find no
strong positive correlation. Instead, a weak negative correlation between L$_{\rm 3.3~PAH}$~
and the optical luminosity seems to be present among PAH-detected objects.
Assuming that the strengths of the 3.3 and 7.7$\mu m$~PAH emissions are correlated,
this result is inconsistent with previous studies \citep[e.g.,][]{ntz07,lutz+08},
which reported a positive correlation between 7.7$\mu m$~PAH luminosity
and 5100\AA~luminosity.
One potential bias is the contribution from host galaxy starlight to L$_{\rm 5100\AA}$
since for low luminosity AGN, such as the sample considered here, the amount
of starlight can be comparable to the AGN flux in the optical range \citep[e.g.,][]{woo06, bennert10}.

To correct for the host galaxy contribution, we measured the nuclear luminosity at 5100\AA~
based on the 2-dimensional AGN-host galaxy decomposition analysis using high-resolution
images obtained with the Hubble Space Telescope (for details, see Treu et al. 2007; Bennert et al. 2010).
The mean AGN-to-total flux ratio of our sample is 0.26 (see Table 1),
indicating that the correction for the host galaxy contribution at 5100\AA~ is necessary.
After correcting for the host galaxy contribution,
we compare the pure AGN optical luminosity at 5100\AA~ with the PAH luminosity
as shown in Figure 3 (right).
The nuclear luminosity (L$_{\rm 5100,nuc}$) becomes significantly smaller than the observed luminosity at 5100\AA.
However, this correction does not significantly change the trend
between L$_{\rm 3.3~PAH}$~and AGN continuum luminosity.

These results are rather contradictory to the previous studies that claimed positive
correlations between AGN activity and various starburst indicators, i.e.,
L$_{\rm 3.3~PAH}$~and far-IR luminosity \citep[e.g.][]{ntz07,Wt08,Oi10}.
Note that there are many Type 1 AGN without PAH detections in the previous studies
as well as our observation.
By including these upper limits,
the correlation between PAH and AGN luminosities can substantially weaken.
On the other hand, since the luminosity range of our sample is rather limited,
we cannot conclude whether or not there is a correlation between L$_{\rm 3.3~PAH}$~and L$_{\rm 5100\AA}$ in a larger luminosity range.

Instead of optical luminosities, we can use X-ray luminosity, which is
a good indicator of AGN activity since X-ray is dominantly radiated from
accretion disk in Type I AGN.
In Figure 4 (left), we compare L$_{\rm 3.3~PAH}$~with AGN X-ray luminosity integrated
over the 0.5 to 8 keV range,
measured from Chandra X-ray images \citep{szathmary11}.
Within the order of magnitude range of the X-ray luminosity,
we see no strong positive correlation.
We also used the bolometric luminosity of AGN determined from multi-wavelength SED fitting
analysis \citep[for details, see][]{szathmary11} to compare with L$_{\rm 3.3~PAH}$. As shown in Figure 4
(right), we see no strong correlation between L$_{\rm 3.3~PAH}$~ and the AGN bolometric luminosity
within the limited range of the observed luminosity.

\begin{figure}
\epsscale{1.2}
\plotone{f4.eps}
\caption{The correlation of $L_{3.3 PAH}$ with X-ray luminosity ($L_{0.5-8 Kev}$)
measured from Chandra X-ray images.
Symbols are same as in Figure \ref{fig3}.
\label{fig5}}
\end{figure}

\begin{figure}
\epsscale{1.1}
\plotone{f5.eps}
\caption{The correlation of nuclear L$_{\rm 3.3~PAH}$~with AGN optical luminosity.
Filled squares represent L$_{\rm 3.3~PAH}$~ measurements from ground-based spectroscopy with
a narrow-slit while open circles represent the estimated nuclear L$_{\rm 3.3~PAH}$~
of the AKARI sample, after dividing by a factor of
$\sim$23, which is the ratio between global and nuclear PAH luminosity of NGC 7469.
\label{fig8}}
\end{figure}

\begin{deluxetable*}{ccccccccccc}
\tablecaption{Nuclear 3.3$\mu m$~PAH luminosity and AGN properties
\label{table3} }
\tablewidth{0pt}
\tablehead{
\colhead{Object}                   &
\colhead{z}                   &
\colhead{log L$_{\rm PAH 3.3}$}            &
\colhead{Ref.}                     &
\colhead{log M$_{\rm BH}$}         &
\colhead{Method}                   &
\colhead{Ref.}                     &
\colhead{log $\lambda$L$_{5100,nuc}$}  &
\colhead{Method}                   &
\colhead{Ref.}                     \\
\colhead{}
&\colhead{}
&\colhead{(erg/s)}
&\colhead{}
&\colhead{(M$_{\odot}$)}
&\colhead{}
&\colhead{}
&\colhead{(erg/s)}
&\colhead{}
&\colhead{}                         \\
\colhead{(1)}                        &
\colhead{(2)}                        &
\colhead{(3)}                        &
\colhead{(4)}                        &
\colhead{(5)}                        &
\colhead{(6)}                        &
\colhead{(7)}                        &
\colhead{(8)}                        &
\colhead{(9)}                        &
\colhead{(10)}                        \\
}
\startdata
NGC 3227               & 0.0039 & 39.36 &  2 &  7.60 & reverberation       & 2         &  42.48  & bulge-disk decomposition  & 2         \\
NGC 4235               & 0.0008 & 39.64 &  1 &  7.71 & single-epoch virial & this work &  42.08  & from L$_{\rm H\alpha}$    & this work \\
NGC 4748 (MCG-2-33-34) & 0.0146 & 40.18 &  1 &  6.39 & reverberation       & 1         &  42.74  & from spectral fitting & 1 \\
NGC 5273               & 0.0036 & 39.30 &  4 &  6.85 & single-epoch virial & this work &  41.45  & from L$_{\rm H\alpha}$    & this work \\
NGC 5940               & 0.0339 & 40.80 &  1 &  7.95 & single-epoch virial & this work &  43.37  & from L$_{\rm H\alpha}$    & this work \\
Mrk 335                & 0.0258 & 40.49 &  1 &  7.13 & reverberation       & 2         &  43.78  & bulge-disk decompositoin & 2      \\
Mrk 509                & 0.0344 & 41.00 &  1 &  8.14 & reverberation       & 2         &  44.16  & bulge-disk decompositoin & 2      \\
Mrk 530                & 0.0295 & 40.88 &  1 &  8.06 & M$_{\rm BH}-\sigma_{*}$~relation    & 3         &  43.71  & from L$_{\rm bol.}$          & 3      \\
Mrk 618                & 0.0356 & 40.85 &  1 &  8.34 & M$_{\rm BH}$-L$_{\rm bulge}$ relation & 4     &  44.03  & from M$_{\rm BH}$ and Eq. 1     & 4      \\
Mrk 766 (NGC 4253)     & 0.0129 & 40.32 &  2 &  6.23 & reverberation       & 1          &  42.81  & from spectral fitting    & 1 \\
Mrk 817                & 0.0315 & 41.00 &  1 &  7.67 & reverberation       & 2          &  43.64  & bulge-disk decomposition & 2 \\
3C 120                 & 0.0330 & 41.04 &  1 &  7.72 & reverberation       & 2          &  44.09  & bulge-disk decomposition & 2 \\
PG 0157+001 (Mrk 1014) & 0.1631 & 42.32 &  3 &  8.31 & single-epoch virial & 5          & 44.89  & spectral fitting         & 5 \\
PG 1211+143            & 0.0809 & 41.43 &  3 &  8.14 & reverberation       & 2          &  44.70  & bulge-disk decomposition & 2 \\
PG 1411+442            & 0.0896 & 41.49 &  3 &  8.63 & reverberation       & 2          &  44.52  & bulge-disk decomposition & 2 \\
PG 1416-129            & 0.1289 & 41.40 &  3 &  8.83 & single-epoch virial & 5          &  44.55  & spectral fitting         & 5 \\
PG 1440+356            & 0.0791 & 41.51 &  3 &  7.80 & single-epoch virial & 6          &  44.54  & spectral fitting         & 6 \\
\enddata

\tablecomments{
Col. (1): Object name.
Col. (2): Redshift.
Col. (3): 3.3$\mu m$~PAH luminosity
Col. (4): reference for L$_{\rm 3.3~PAH}$.
1. \citet{imanishi04}.
2. \citet{Rod03}
3. \citet{imanishi11}.
4. \citet{Oi10}.
5. \citet{imanishi10}.
Col. (5): Black hole mass
Col. (6): reference for black hole mass
1. Bentz et al. (2009b).
2. Peterson et al. (2004).
3. Nelson \& Whittle (1995).
4. Ryan et al. (2007).
3.
Col. (7): AGN monochromatic luminosity at 5100\AA,
Col. (8): reference for L$_{5100}$.
1. Park et al. (2011).
2. Bentz et al. (2009a).
3. Woo \& Urry (2002).
4. Ryan et al. (2007).
5. Ho \& Kim (2009).
6. Shang et al. (2007).
}

\end{deluxetable*}

\subsection{Nuclear PAH emission and AGN activity}

In this section, we investigate how the nuclear 3.3$\mu m$~PAH emission
is related to AGN activity. We collected from the literature
all 3.3$\mu m$~PAH measurements of Type I AGN, for which AGN luminosity
and black hole mass can be compared. We found 3.3$\mu m$~PAH measurements
for 20 local Seyfert 1 galaxies and PG QSOs based on the previous
ground-based long-slit observations \citep{Rod03,imanishi04,Wt08,Oi10,imanishi11}.
These measurements based on the long-slit spectroscopy with a narrow slit
represent the strength of the nuclear 3.3$\mu m$~PAH emission.
Except for 3 AGN without necessary measurements of AGN properties in the literature,
we determined black hole mass and AGN continuum luminosity at 5100\AA.
Thus, we have a sample of 17 local Type I AGN as listed in Table 3.

For black hole masses, we adopted the reverberation mapping measurements
from Peterson et al. (2004) and Bentz et al. (2009b), after calibrating
with the most recent determination of the virial factor from \citet{woo10}.
When reverberation mapping results were not available, we used the single-epoch
virial method as used for the moderate-luminosity AGN sample.
In practice we use the following equation to estimate black hole masses (Park et al. 2011):
\begin{equation}
M_{\rm BH} = 10^{7.602}{\rm M}_{\odot} \left(
{\sigma_{{\rm H}\beta}({\rm rms}) \over 1000~ {\rm km~s}^{-1} } \right)^{2} \left( {\lambda
L_{5100,nuc} \over 10^{44}~ {\rm erg~s}^{-1}} \right)^{0.518}~,
\label{eq:MBH_sigmaRMS}
\end{equation}
where $\sigma_{\rm H\beta}$ is the line dispersion of the H$\beta$~line and L$_{5100, nuc}$
is the AGN continuum luminosity at 5100\AA~corrected for the host galaxy starlight contribution.
For NGC 4235, NGC 5273, and NGC5940 with no line width measurements in the literature,
we fit the broad H$\alpha$~ emission line and measured the line width and luminosity
using the spectra from the Sloan Digital Sky Survey.
For two objects (Mrk 530 and Mrk 618) without any available spectra,
we used the black hole mass -galaxy property relations, i.e., M$_{\rm BH}-\sigma_{*}$ and
M$_{\rm BH}$-L$_{\rm bulge}$ relations \citep{gultekin+09} to calculate black hole masses
(see Table 3 for details).

In the case of AGN power, we collect AGN continuum luminosity
at 5100\AA~as a proxy for the bolometric luminosity of AGN.
For high luminosity QSOs, i.e., PG QSOs, it is not necessary to correct
for the host galaxy starlight contribution. In contrast, for low luminosity AGN,
L$_{\rm 5100\AA}$ should be corrected for the host galaxy contamination.
In general we obtained L$_{\rm 5100\AA, nuc}$ measurements from previous studies,
which were based on either bulge-disk decomposition analysis using HST images or
spectral fitting analysis using high quality spectra. For 3 objects, namely NGC 4235, NGC5273,
and NGC 5940, we determined AGN continuum luminosity from H$\alpha$~line luminosity
using the tight correlation between L$_{5100 \AA,nuc}$ and L$_{\rm H\alpha}$
\citep[see Eq. 1 and 2 in][]{greene&ho05}.

In contrast to the ground-based observations, L$_{\rm 3.3~PAH}$~ measured from AKARI observations represents the global starburst as discussed in \S~3.1.
Thus, in order to include the PAH emission measurements from AKARI
observations, it was necessary to calibrate them for representing nuclear
starburst. The relation between nuclear and global starburst for Type I AGN
has not been studied in detail \citep{imanishi10}. Although the
nuclear-to-global starburst ratio can vary for individual objects,
we used the case of NGC 7469 to estimate the difference.
As discussed in \S~3.1, NGC 7469 was observed with a ground-based spectrograph
with a narrow-slit and the AKARI IRC, respectively.
The flux ratio between nuclear L$_{\rm 3.3~PAH}$~ and the upper limit of the global L$_{\rm 3.3~PAH}$~is $\sim$0.04.
Thus we took this ratio as a calibration factor and scale down the AKARI
measurements by a factor of 0.04.

In Figure 5, we present the correlation between
the nuclear 3.3$\mu m$~PAH luminosity and AGN optical luminosity at 5100\AA~
for the combined sample.
The Type I AGN from ground-based observations clearly show a correlation,
suggesting the nuclear starburst-AGN connection. The L$_{\rm 3.3~PAH}$~of
the moderate-luminosity AGN at z$\sim$0.4, which are calibrated for representing
the nuclear PAH emission, are consistent with the trend found by
nuclear L$_{\rm 3.3~PAH}$~measurements although they are more scattered probably
due to the uncertainty of the calibration.

Using the nuclear L$_{\rm 3.3~PAH}$~measurements from ground-based spectroscopy,
we fit the relation between L$_{\rm 3.3~PAH}$~and AGN luminosity.
Since most of the L$_{\rm 3.3~PAH}$~measurements in the literature do not have error estimates,
we fit the best-slope without accounting for the measurement uncertainties.
The best-fit relation is:
\begin{equation}
\log ({\rm L_{\rm PAH 3.3} \over 10^{41}~ {\rm erg s^{-1}}}) = 0.06\pm0.01 + (0.77\pm0.01)
\times \log ({\rm L_{\rm AGN~5100\AA} \over 10^{44}~ {\rm erg s^{-1}}}).
\label{eq:msigma}
\end{equation}
The best-fit slope of $\sim$0.8 indicates that the correlation is not linear.
This implies that for higher luminosity AGN, the nuclear starburst-to-AGN luminosity
ratio is smaller, albeit with the small sample size.

In Figure 6, we compare nuclear L$_{\rm 3.3~PAH}$~with the Eddington ratio and black hole mass
to test whether the accretion rate and black hole mass correlates
with starburst activity.
We estimate the Eddington ratio by multiplying a factor
of 9 to the AGN optical luminosity.
In the case of the Eddington ratio, there is a general trend that higher
Eddington ratio objects show higher nuclear starburst activity although
there is a large scatter.
Black hole mass shows a similar trend with L$_{\rm 3.3~PAH}$~in that the host galaxies
of higher mass AGN show higher nuclear starburst luminosity. This can
be interpreted as the trend that higher mass AGN in the sample are
generally higher luminosity AGN, i.e., PG QSOs. Thus, the relation
between black hole mass and PAH luminosity reflects the correlation
between AGN power and L$_{\rm 3.3~PAH}$.

\begin{figure}
\epsscale{1.2}
\plotone{f6.eps}
\caption{Correlation of nuclear L$_{\rm 3.3~PAH}$~with AGN optical luminosity.
Filled squares represent L$_{\rm 3.3~PAH}$~measurements from ground-based spectroscopy with
a narrow-slit while open circles represent the estimated nuclear L$_{\rm 3.3~PAH}$~
of AKARI sample, after dividing by a factor of
$\sim$23, which is the ratio between global and nuclear PAH luminosity
of NGC 7469.
\label{fig6}}
\end{figure}

\section{Discussion and Conclusions}

To investigate the starburst-AGN connection, we compared
the global and nuclear 3.3 $\mu m$~PAH emission with AGN
luminosity using a sample of Type I AGN.
The global 3.3 $\mu m$~PAH emission luminosities are measured
for moderate-luminosity AGN at z$\sim$0.4,
based on our new AKARI slit-less spectroscopy, which covers the
entire host galaxies.
We find no strong correlation between 3.3 $\mu m$~PAH and AGN optical
luminosities within the limited AGN luminosity range 10$^{44}$ - 10$^{45}$ erg s$^{-1}$.
This result may imply that the global star formation is not strongly
related with AGN activity although we cannot rule out a weak correlation
with a considerable scatter. We note that since the AGN luminosity range
is very limited, whether the global star formation rate
correlates with AGN activity is inconclusive.

In contrast, when we compare AGN luminosity of the local Seyfert 1 galaxies
and PG QSOs with their nuclear 3.3 $\mu m$~PAH emission luminosity,
we detect a strong correlation,
suggesting that that AGN activity is related to the nuclear starburst.
These results are consistent with the findings of previous studies on the starburst-AGN
connection \citep{Im03, imanishi04, ntz07, lutz+08, Oi10}.

The slope of the L$_{\rm 3.3~PAH}$~correlation with AGN luminosity in Figure 5 shows
that the L$_{\rm 3.3~PAH}$~to AGN luminosity ratio decreases toward higher AGN luminosity.
At face value, it implies that the nuclear starburst activity
is slightly suppressed in the host galaxies of high luminosity AGN (for different predictions
on the starburst-to-accretion ratios, see e.g., Kawakatu \& Wada 2008; Ballantyne 2008).
A similar trend was noted by \cite{lutz+08} in comparing 7.7 $\mu m$~PAH emission
and AGN luminosities.
In their study, high luminosity AGN with L$_{\rm 5100\AA}$ $>$ 10$^{46}$ erg s$^{-1}$~
show a much lower starburst-to-AGN ratio \citep[see Figure 6 in][]{lutz+08},
implying that the black hole growth rate normalized by the starburst rate is a factor of
10 higher in their high redshift QSOs than in the local AGN.
In our local sample the decrease of the starburst-to-AGN ratio with increasing
AGN luminosity is not as dramatic as in high redshift QSOs, but if confirmed,
it implies that for low-luminosity AGN
the growth of galaxy centers is faster than black hole growth in the present-day universe.
However, it is not clear whether black hole growth is slower or faster than the total host
galaxy growth since only nuclear starbursts are compared in our analysis.

We note that there are many AGN with no PAH emission detection.
Including the upper limits of
these objects significantly weakens the correlation between L$_{\rm 3.3~PAH}$~and AGN luminosity.
Although the true PAH luminosities of these objects may be close to the upper limits
within a factor of few, a detailed investigation using a large sample with lower
flux limits is necessary to probe the slope and scatter of the correlation.

\acknowledgements
This work has been supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (MEST), No. 2010-0021558.
M.I. acknowledges support by Grants-in-Aid for Scientific Research no. 22012006.
This research is based on observations with AKARI, a JAXA project with the participation of ESA.

redpajama_set_name: RedPajamaArXiv


text:
Ontelly
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1968 The Sixty-Eighters at Sixty
David Aaronovitch assesses the legacy of 1968, talking to the self-styled revolutionaries of 40 years ago
1968 The Sixty-Eighters at Sixty - Episode 1
David Aaronovitch assesses the legacy of 1968, talking to the self-styled revolutionaries of 40 years ago. He talks to Foreign Office minister Kim Howells, then a leader of the Hornsey Art College occupation. Feminist Sheila Rowbotham recalls the communal house she was living in. John Birt explains why his rigorous reforms as BBC director general followed on from his youthful anti-establishment views. Right-wing columnist Bruce Anderson talks about his youthful communist self and why he changed, partly as a result of the conflict in his native Northern Ireland Finally, David visits Northern Ireland itself to explore the outcome of the civil rights movement and the aggression it provoked, now seen by many as a crucial step in Ulster's descent into violence.
David Aaronovitch assesses the legacy of 1968, talking to the self-styled revolutionaries of 40 years ago. Visiting Berlin, he talks to former rebel Thomas Schmid, now a senior editor with Springer newspapers. Educationalist Katharina Rutschky explains how a movement which produced the brutality of the notorious Baader-Meinhof gang also paved the way for a revolution in childcare. Other contributors include novelist Peter Schneider and Green MP Marie-Luise Beck.

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Summary Sentence: The Georgia Tech campus community is invited to hear from Institute leadership on fostering a campus culture of ethics and integrity in order to preserve the public trust.
Full Summary: The Georgia Tech campus community is invited to hear from Institute leadership on fostering a campus culture of ethics and integrity in order to preserve the public trust.
The Georgia Tech campus community is invited to hear from Institute leadership on fostering a campus culture of ethics and integrity in order to preserve the public trust.
Keynote speaker, President G. P. "Bud" Peterson will talk about the importance of cultivating character and understanding the difference between acting in compliance and acting ethically in our complex environment.
This event is part of Ethics Awareness Week. Learn more at gatech.edu/about/ethics.


#funkyfriday — A Tribe Called Quest / "Check the Rhime (Scott Nice Remix)"
Scott Nice nails this mashup of an ATCQ classic with an old school Havana vibe. The perfect funky introduction to your nice weekend.
Enjoy this track, and the weekend. See you here for #musicmonday.
#musicmonday — Anchorsong / "Slider"


text:
A final look at ESPN's Playoff Predictor ahead of selection committee's final rankings
Mark Schipper | 26 days ago
On the Sunday morning following the season's final Saturday college football is deep into the countdown for both the bowl game matchups and College Football Playoff selections to be revealed.
With just hours left before the future officially is written, ESPN Stats and Info has released their final Allstate Playoff Predictor rankings, and their projections are what many assumed would be the case, and many others feared.
Out of the Big Ten, the 6-0 Ohio State Buckeyes are an 89.3 percent certainty to make the final four, trailing only undefeated 11-0 Alabama and well ahead of 83.8 Clemson at 10-1. This was expected and not a surprise in the least. Despite the Buckeyes playing barely half the amount of games of the rest of the country, they entered the season a playoff favorite and never relinquished their post.
"Even though Ohio State only played six games, going 6-0 against that schedule was an accomplishment," the Stats and Info release stated. "In fact, Ohio State ranks 4th in Strength of Record, ahead of Clemson, Cincinnati and Oklahoma. Plus, the Buckeyes were ranked 4th by the committee last week and won the Big Ten Championship this week."
The Notre Dame Fighting Irish, despite yet another championship game blowout loss, this time a 34-10 bludgeoning to likely playoff bound Clemson, are by far the most likely pick at the number four spot, according to Stats and Info.
The Irish are at 66.8 percent likelihood of being selected, while the next closest, Texas A&M, is at 33.6 percent despite their big road win over Tennessee to end the season and finish up 8-1. If the Irish go fourth to Alabama's expected number one, it would set up a rematch of the 2012 BCS national championship, a game Alabama won 42-14 down in Miami Gardens, Florida.
Those are the predictions and ESPN Stats and Info is sticking to them. The official selections will be known before the day is out.
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Mark Schipper
Mark Schipper is a reporter, sportswriter, and aspiring novelist living in Chicago, Illinois.
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text:
Alcina Dimitrescu , mieux connue sous le nom de Lady Dimitrescu, est un personnage fictif du jeu vidéo de survival horror Resident Evil Village, publié par Capcom en 2021. Antagoniste parmi les plus importants de Village, elle est présentée comme une aristocrate géante aux traits de vampire. Elle réside avec ses trois filles au château Dimitrescu, sa forteresse située à proximité du village roumain éponyme où s'aventure le protagoniste Ethan Winters. Dimitrescu gouverne le village aux côtés de trois seigneurs mutants, sous la supervision d'un chef suprême connu sous le nom de Mère Miranda.

Dès les avant-premières et les démos de Village publiées par Capcom entre fin 2020 et début 2021, Lady Dimitrescu a, de manière inattendue, gagné en popularité à l'international et fait l'objet de quantité de créations de fans, comme des fan arts, des cosplays, des mèmes et des œuvres érotiques. Des journalistes et commentateurs ont relevé cette tendance, qui a commencé bien avant la sortie de Village le 7 mai 2021, et ont attribué la montée rapide de l'intérêt des fans pour le personnage à divers aspects de son apparence et à son sex-appeal. Cependant, malgré cet accueil populaire, de nombreux fans et critiques ont été déçus par le peu de temps d'écran qui lui est alloué.

Concept et création
Créée par Capcom pour le jeu vidéo Resident Evil Village, Lady Dimitrescu est née du désir de créer un personnage de femme fatale charismatique.  Elle est conçue pour être l'archétype du maléfique « vampire envoûtant », le développeur souhaitant revisiter les racines survival horror de la franchise Resident Evil. Le nom Dimitrescu se prononce Dimitrisk, la lettre finale « u » étant silencieuse.  Le personnage est inspiré de l'aristocrate hongroise du  Élisabeth Báthory, de la légende urbaine japonaise de Hasshaku-sama (ou Hachishaku-sama) reprise comme histoire de fantômes sur internet, ainsi que de la représentation d'Anjelica Huston en tant que Morticia Addams dans la famille Addams. Certaines caractéristiques de Lady Dimitrescu font également référence à Ramon Salazar de Resident Evil 4, un antagoniste secondaire qui avait marqué de nombreux joueurs comme adversaire mémorable.

Selon Tomonori Takano, le directeur artistique de Resident Evil Village, l'équipe de développement s'éloigne volontairement des éléments simplistes comme les zombies, et crée plutôt des situations uniques et des personnages mémorables qui suscitent la peur d'une nouvelle manière, poursuivant ainsi la démarche entamée dans Resident Evil 7: Biohazard, le prédécesseur de Village. Boss de la zone du château Dimitrescu, Lady Dimitrescu apparaît comme une ennemie presque invulnérable, aux longues griffes acérées et rétractables. Dimitrescu est programmée pour traquer le personnage jouable Ethan Winters dans tout son château ; elle est censée être constamment évitée par le joueur, tout comme M. X de Resident Evil 2 et son remake de 2019, ou comme les membres de la famille Baker de Resident Evil 7.

Dimitrescu commande ses « filles » Bela, Cassandra et Daniela comme ses subordonnées. Produits de ses expériences avec le parasite Cadou, leurs corps sont composés de mouches qui s'agrègent sous la forme des cadavres dévorés et ne peuvent se former que dans les murs du château. Le Château Dimitrescu est à l'origine imaginé comme étant habité par « des dizaines et des dizaines » de filles de Dimitrescu, mais la famille a finalement été réduite à Alcina Dimitrescu et ses trois filles à l'issue des tests sur le rythme du jeu. Dimitrescu et ses filles, qui se disputent l'attention et l'approbation de leur mère, se nourrissent de sang humain ; les restes de leurs victimes masculines sont crucifiés et exposés à l'extérieur du Château Dimitrescu. On dit que Dimitrescu fait preuve d'une attitude protectrice très maternelle envers ses filles, ce que les développeurs laissent entendre en présentant son histoire comme parallèle à celle de la propre famille d'Ethan, que celui-ci tente également de protéger.

Dimitrescu mesure  de haut, en prenant en compte son chapeau et ses talons hauts. Comme Takano voulait éviter les images gothiques typiques associées aux anciens jeux Resident Evil et au genre horrifique dans son ensemble, le design visuel des Dimitrescu fait à la place référence aux tendances de la mode des années 1930. Les vêtements finement brodés des trois sœurs arborent les armoiries aux motifs floraux de la famille Dimitrescu. Lady Dimitrescu apparaît tout d'abord dans un premier prototype qui utilise le modèle de l'épouse d'Ethan, Mia Winters de Resident Evil 7, mais avec un chapeau et une robe, ce qui lui a donné une apparence fantomatique, mais pas suffisamment effrayante. L'équipe a donc augmenté l'échelle du modèle dans le jeu et remarqué qu'avec les accessoires, l'effet était bien là. Sur la base de ce prototype, l'une des premières images conceptuelles de Lady Dimitrescu dessinée par Takano impliquait son visage imposant se penchant pour franchir une porte et lui conférait presque trois mètres de hauteur, ce qui, selon lui, devait faire l'objet d'une scène dans la version finale du jeu, en plus d'être présent dans le premier trailer.

Apparitions
Son passé reste largement un mystère, Dimitrescu a hérité d'une hémopathie avant de rencontrer Miranda, qui l'a infectée avec le parasite Cadou dans le but de voir si elle était compatible avec son ambition de ressusciter sa fille. Bien que dotée d'excellentes capacités de régénération et d'une vie éternelle, la maladie de sang préexistante d'Alcina l'obligeait à ingérer régulièrement de grandes quantités de sang et de chair humaine pour maintenir son état, augmentant sa taille et engendrant ses « filles » Daniela, Bela et Cassandra. La famille Dimitrescu était étroitement associée aux familles nobles Beneviento, Moreau et Heisenberg, entretenant avec elles une alliance pour contrôler la région. Cette mainmise a permis à la famille Dimitrescu de régner sur son château avec une cruauté barbare, employant régulièrement du nouveau personnel pour remplacer ceux qui étaient emmenés dans le donjon, tués et utilisés pour créer un vin rouge enrichi à partir de leur sang.

Ethan Winters a été capturé par les filles de Dimitrescu et accroché à un mur pour être vidé de son sang, mais il parvint à se libérer et à tuer les filles une à la fois. Exaspérée, Alcina décide d'ignorer les ordres de Miranda et entreprend de tuer Ethan elle-même. Forcée alors de muter pour prendre sa forme réelle de dragon, elle affronte Ethan dans la crypte familiale de son domaine et, finalement, meurt de sa main.

Promotion commerciale et marchandise
Pour promouvoir Resident Evil Village, Capcom a distribué des figurines grandeur nature de Lady Dimitrescu dans les magasins de jeux vidéo. À Hong Kong, du matériel promotionnel mettant en vedette le personnage a été affiché dans les transports en commun au début de l'année 2021.  Parmi les marchandises notables présentant le personnage, on peut voir des serviettes grandeur nature qui ont été offertes comme prix aux participants japonais d'un concours organisé sur Twitter. La cosplayeuse professionnelle Yaya Han a publié une vidéo sponsorisée par Capcom sur sa chaîne YouTube, qui documente le processus derrière ses cosplays du personnage en avril 2021. Le 30 avril 2021, une mini-série de marionnettes mettant en vedette Dimitrescu aux côtés de ses pairs a été diffusée sur la chaîne YouTube officielle biohazard. Son image a été reprise par des marques tierces telles que Domino's Pizza Malaysia pour promouvoir leurs produits.

Accueil
Lady Dimitrescu a reçu un accueil très positif de la part des critiques et des joueurs après son apparition initiale dans une bande-annonce promotionnelle pour Resident Evil Village dévoilée en 2020, et pour son apparition dans la démo exclusive PlayStation 5 Maiden publiée le 21 janvier 2021. En février 2021, Takano a publiquement reconnu ce qu'il a décrit plus tard comme une réponse étonnamment enthousiaste au personnage. Même si le lancement de Village était prévu pour le 7 mai 2021, la montée en popularité de Dimitrescu au début de 2021 a conduit à une importante exploitation de l'image du personnage à travers le fan art ; recevant une publicité faite par des fans eux-mêmes, par des individus notables tels que Han ou la médaillée de bronze olympique Ekaterina Lisina; et les mèmes Internet, qui impliquaient parfois la participation d'autres développeurs de jeux vidéo sur les réseaux sociaux. Dimitrescu a fait l'objet de mods de jeux vidéo réalisés par les fans ; comme un mod pour Fallout 4 qui recrée sa robe ivoire à manches longues pour être portée par le personnage du joueur, ou un mod pour Village qui remplace le visage de Dimitrescu par celui de Thomas the Tank Engine, Eurogamer le décrivant comme « l'acte phare » des « mods florissants de la scène » du jeu. En mars 2021, dans une liste de personnages et de marques inclus dans une enquête distribuée aux joueurs de Fortnite, Epic Games a inclus Lady Dimitrescu aux côtés des protagonistes de la série, Jill Valentine et Ethan Winters, afin d'évaluer l'intérêt pour de futures promotions crossover.

Plusieurs commentateurs ont longuement discuté du phénomène derrière la popularité du personnage, beaucoup identifiant sa taille inhabituellement grande comme élément-clé de l'intérêt des fans. Leon Hurley de GamesRadar+ a constaté que Dimitrescu n'est pas le méchant principal de Village ou son personnage le plus important, mais qu'il est néanmoins devenu plus important, populaire, discuté et reproduit que ce qui était initialement prévu ou envisageable. À la lumière de l'accueil positif du personnage, Jess Kinghorn, de GamesRadar+ également, a suggéré que l'industrie du jeu vidéo devrait être moins obsédée par la jeunesse, et mettre en vedette des personnages féminins plus âgés à la caractérisation approfondie.

Certains commentateurs ont suggéré qu'une partie de l'intérêt des fans pour le personnage est de nature érotique ou sexuelle, et plus particulièrement lié à la domination féminine. La popularité de Dimistrescu a en effet inspiré une quantité importante de pornographie et de fétichisme sexuel ou érotique chez les fans. Le personnage aurait notamment suscité un certain intérêt pour le piétinement, l'acte d'être piétiné par un partenaire jouant un rôle sexuellement dominant. L'écrivaine érotique professionnelle Gemma Glitter a attribué une part de l'intérêt pour le personnage à la macrophilie, dans ce cas une fascination pour les femmes de taille gigantesque. Steven T. Wright de Input Mag a rapporté que le sex-appeal de Lady Dimitrescu représente la fétichisation de la hauteur de leur corps pour plusieurs femmes de grande taille bien réelles, car elle est considérée comme « à la fois un symbole de leur propre pouvoir et de leur allure, et un rappel douloureux des stigmates sociaux complexes que la société attache au corps de la femme ».

Notes et références

Notes

Références

Boss de jeu vidéo
Personnage de Resident Evil
Personnage de fiction roumain
Cannibale de fiction
Personnage féminin de jeu vidéo

redpajama_set_name: RedPajamaWikipedia


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Maid of the Mist Electric Ferries
Maid of the Mist launched two new-generation all-electric passenger ferries for the tour of Niagara Falls in the US.
Electric passenger ferries
Service Entry
Contractors Involved
ABB, Propulsion Data Services, Burger Boat Company
Maid of the Mist electric ferries entered service in October 2020. Credit: ABB.
The zero-emission ferries have been christened James V Glynn and Nikola Tesla in honour of the Maid of the Mist chairman, and the well-known energy pioneer, respectively.
The new electric vessels were built as a part of the $70m revitalisation initiative of Niagara Falls State Park, which also involves the renewal of the park's major viewing areas.
The vessels entered service in October 2020. Maid of the Mist vessels operate from April through the first week of November. The vessels leave from their downstream dock to the base of Niagara Falls every 30 minutes and serve approximately 1.6 million guests annually.
Maid of the Mist background
Maid of the Mist has been providing tour services at the Niagara Falls waterfalls and the Niagara River Gorge for more than 100 years.
The first Maid of the Mist steamboat completed its maiden voyage between the US and Canada in 1846. The Maid of the Mist was re-branded as a tourist sightseeing service provider, after the construction of a suspension bridge between the countries in 1848.
The first diesel-powered steel-hulled Maid of the Mist vessels were introduced in 1955. In 2018, the company started research to replace diesel boats with electric propulsion.
In May 2019, Maid of the Mist announced the construction of two new emission-free vessels to make the New York State a premier environment-friendly tourism destination.
The two new electric vessels replaced the Maid of the Mist VI (1990) and Maid of the Mist VII (1997) diesel-powered vessels in the fleet. Both the vessels had the capacity to carry 600 passengers.
Maid of the Mist electric ferries design and features
The new 28m-long catamaran-style electric vessels feature twin hulls made of 5086 H116 marine-grade corrosion-resistant aluminium alloy. The two independent power systems on board the vessel help in increasing the resilience of operations by generating redundancy.
The wide stance offers a smooth and quiet ride to passengers and also allows them to better enjoy Niagara Falls.
The new boats provide more space and comfortable ride to its passengers. The modular vessel further integrates ABB's zero-emission technology and generates no exhaust fumes, engine noise and vibrations.
Propulsion and power
The ferries are powered by a pair of 316kWh lithium-ion battery packs placed across the two hulls. The batteries supply power to the electric propulsion motors that can generate up to 400kW output, controlled by ABB's power and energy management system (PEMS). The system controls the power distribution according to the energy usage onboard.
Each trip consumes approximately 38kWh power. The lithium-ion batteries of the vessels can be recharged in seven minutes, using locally generated hydroelectricity, during the embarking and disembarking of passengers at the dock.
New York State Parks, the New York Power Authority partnered with Maid of the Mist, and ABB to launch the first all-electric vessels in the US.
The vessel was designed by Propulsion Data Services, while Burger Boat Company was responsible for the construction.
ABB supplied switchboards, drives and the integrated power and propulsion system, as well as an onshore charging system. It also provided Ability Marine Remote Diagnostic System for remote equipment monitoring and predictive maintenance, as well as installed the ship-to-shore battery charging connection.


Our most popular bread. A hearty crusty bread made with dark wheat flour. Available plain (Dark) or rolled in seeds (Rustic). Ingredients: dark wheat flour, wheat sourdough, rye flour, barley flour, rye malt, yeast & salt.


I watched the movie,"Contact", once again. I believe it's the fourth time now, but it's possibly more.
Without going into the movie, it basically about a radio transmission discovered by SETI, Dr. Eleanor Arroway (played by favourite actress Jodie Foster) who finds a message within unmistakeable pulses of radio waves. They quickly discover, the radio transmissions are coming from the brightest star,Vega, within the Lyra constellation.
Not long after this intriguing discovery, the founder of keeping the project alive, billionaire S.R. Hadden, provides Eleanor with hidden inside mechanical drafting plans. This leads to constructing a space-age device with a flight pod. It's believed this pod will provide them access to space travel by means of wormholes.
After a series of conflicts and failures, Dr. Arroway is zipped through space and time, while on earth only a few seconds of time pass by, but to Eleanor 18 hours quickly disappear.
It's science-fiction and indeed a movie to add to your list, if you haven't seen it yet.
To me, "Contact" sparked another interesting concept of space travel.
Consider, if you may, what if we could travel across the Cosmos without leaving earth at all.
By means of "holographic projection" of ourselves.
With exoplanets approximately 500 light years away, it would still take over 8 million years at the speed of light, (17500 years to reach one light-year) before even reaching one of these planets. But say we could propel our image faster then the speed of light by folding space and time.Theoretically our holographic-selfs could explore our vast universe, reaching M-source-Planets.
Just imagine the implications of such a trip?
Is it just a dream or maybe a real vision into the future? Scientists would surely dispute my claims, rationalizing with their mathematical calculations, but a dream is the start of a vision.
Will mankind be the Leaders of Space Exploration on a universal scale?
Only time will tell. Maybe it's time to remove the "time-factor" from the equation by folding it into space.
It's time to think outside the box and reach for the stars by using Time Travel.
LOGLINE: Young Hunter goes missing deep within British Columbia's rugged wilderness, only to be hunted by an 800 lb Grizzly.
My screenplay "Missing Up North – Bloody Survival" is based on a true story around the mis-adventures of 20 year old Hunter named Rivers, who went missing in the wild mountainous Chilcotin region by Williams Lake, B.C. for over 16 hours, hunted down by a savage Grizzly.


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A supporter of Iran's Supreme Leader Ayatollah Ali Khamenei waves an Iranian flag while attending a gathering at the Azadi soccer stadium in west Tehran on May 26, 2022. Protesters often wave a version of this flag without its tulip motif to signal opposition to the government.
Photograph By Morteza Nikoubazl, NurPhoto/Getty Images
Why Iran's flag is at the center of controversy at the World Cup
In 1980, the newly installed Islamic Republic replaced the Lion and Sun on the country's tricolor flag with a tulip-shaped emblem—making both into potent political symbols.
ByAmy McKeever
Iran has been in turmoil since the September death of 22-year-old Mahsa Amini, who had been in the custody of Iran's morality police. Months of upheaval and demonstrations for women's rights in Iran have spilled over into an unlikely place—the soccer pitch at the World Cup.
Last week, Iranian fans carrying the country's pre-revolutionary flag were barred from attending its game against England. Then the U.S. Soccer Federation sparked a firestorm when it displayed Iran's flag on its social media accounts without its iconic tulip emblem.
(5 things to know about Qatar, the 2022 World Cup hosts.)
Modified versions of Iran's tricolor flag have long been used in Iran and its diaspora, both among those who protest the regime's human rights violations and those who are nostalgic for the time before the revolution. Here's what you need to know about the flag and the potent meaning of its motifs.
The colors of the flag
Both the official Iranian flag and the pre-revolutionary flag that is sometimes flown in protest share horizontal stripes of green, white, and red.
These colors are laden with symbolism. Green—believed to be Prophet Muhammad's favorite color—represents Islam and adorns the flags of several Muslim countries, including Pakistan, Saudi Arabia, and Algeria. White is linked to freedom, writes British journalist Tim Marshall in A Flag Worth Dying For, and red is associated with "martyrdom, bravery, fire, and love."
Although these colors had been used in early versions of the banner, the Iranian tricolor flag was officially enshrined in the Constitution of 1906.
The meaning of the flag's emblem—and why it changed
The tulip motif at the center of today's flag is a relatively new addition—and took the place of one of Iran's most beloved emblems, the Lion and Sun, or Shir o Khorshid.
The Lion and Sun symbol dates back to 12th century Persia, where it gained popularity as an ancient astrological sign of the sun in the house of Leo—which likely represented power and royalty. Over subsequent centuries, the Lion and Sun adorned the country's flag in various configurations—at times a symbol of the two pillars of society, the state and religion, or as a symbol of the monarchy.
(History's first superpower sprang from an ancient Iran.)
In 1979, however, the Iranian Revolution overthrew Shah Mohammad Reza Pahlavi and abolished the monarchy. The new leaders of the Islamic Republic turned to architect Hamid Nadimi to come up with a flag design that Marshall writes would "signify a break with the era of the shah, but at the same time reassure an ancient culture that this was not Year Zero."
Nadimi's solution was to replace the Lion and Sun in 1980 with a red tulip—which had long been important in Shia Islam as a symbol of Husayn Ibn Ali al-Hussein, Muhammad's grandson who died a martyr during a 7th century battle. This tulip is comprised of four crescent-shaped petals and one stem, or sword, that form the word Allah and symbolize the five pillars of Islam.
Nadimi also added a stylized Arabic inscription of the words Allahu Akbar, or God is great, across the bottom of the flag's green stripe and across the top of its red stripe.
(See the evolution of over 2,000 world flags in under 5 minutes.)
Modern flag protests
Activists have since used variations of Iran's tricolor flag to signal their resistance to the Islamic Republic. During the 2009 Green Movement, for example, pro-democracy advocates displayed an emblem-free version of the flag in an act of defiance against the ideology of their government.
Although displaying the Lion and Sun is illegal in Iran, it remains for many a nostalgic symbol of the pre-revolutionary era. In 2015, a correspondent for The Guardian spotted the illicit Lion and Sun on "countless pendants, rings, and wall hangings" during a visit to a Tehran bazaar. Some protesters also display the flag to call for a return to the monarchy.
Now, the flag has become a flashpoint once again the recent demonstrations over the death of Mahsa Amini—both on the streets of Tehran and at the World Cup.


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THE MURDER OF EDWIN DROOD: RECOUNTED BY JOHN JASPER, BEING AN ATTEMPTED SOLUTION OF THE MYSTERY BASED ON DICKENS'S MANUSCRIPT AND MEMORANDA.
By Percy T. Carden and Charles Dickens.
C. Palmer.
Online HERE, HERE, and HERE.
Fifty years after Dickens's death and a solution at last! Yeah, sure. A brief excerpt:
It is probably now possible to say that everything emanating directly or indirectly from Dickens in connection with the story is known. Mr. Carden has, however, gone considerably further than this, in that with vivid imagination and not a little literary skill he has sketched out a solution of the story upon entirely novel and highly interesting lines. Starting from the hint given by Forster that the originality of the story was to have been a review of the murderer's career told by himself as if not he, but some other man, were the tempted, Mr. Carden has constructed, largely from Dickens's own materials, a series of episodes, in which he very skilfully propounds his own solution of some of the problems in which the fragment abounds. Whatever opinion may be entertained as to the success of his efforts, no doubt can be felt that he has stated his case forcibly and ingeniously, and the novelty of his method, combined with his considerable literary skill, render his book both interesting and exciting. — Unsigned, "A New Solution of 'Edwin Drood'," THE LIVING AGE (February 12, 1921)
- The New York Times review (January 30, 1921), reproduced at DROODIANA.ru.
- Previous DROOD-related ONTOS articles HERE and HERE.


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Weekend binge-watch list for this week!
Veera Jain
Home › Blogs › Weekend binge-watch list for this week!
Another weekend, same problem- WHAT TO WATCH? Honestly, OTT platforms are always in a hurry and competing to bring the best content. Every month, multiple films and web series are released on the OTT platforms. The new things to watch and spend your weekend are here and we are here to update your list with the Weekend Binge-watch list.
Suzhal on Amazon Prime
Suzhal: The Vortex is a Tamil-language crime thriller web series created by Pushkar–Gayathri for Amazon Prime Video, directed by Bramma G and Anucharan Murugaiyan, and produced by Wallwatcher Films. The series stars Kathir, Aishwarya Rajesh, R. Parthiban, and Sriya Reddy. The first season of the web series consists of eight episodes and it started streaming on 17 June 2022. The web series is set in the fictional town of Sembaloor set in Tamil Nadu, the series is an investigation into the case of a missing person which unravels and rips the intricate social fabric of the small town.
Man vs. Bee on Netflix
Man vs. Bee is a British comedy streaming television series created and written by the famous Rowan Atkinson and William Davies, directed by David Kerr. It stars the famous Atkinson, Jing Lusi, Claudie Blakley, Tom Basden, Julian Rhind-Tutt, Greg McHugh, and India Fowler. The series premiered on Netflix on 24 June 2022. A house sitter named Trevor finds himself entrenched in an ongoing battle with a bee while in the midst of lodging an elegant mansion. The Mr. Bean actor surely has some laughter in the bag for you.
Also Read: Five North East movies you can watch online!
The Umbrella Academy Season 3 on Netflix
The Umbrella Academy is an American superhero streaming television series based on the comic book series of the same name written by Gerard Way, illustrated by Gabriel Bá, and published by Dark Horse Comics. The show is created for Netflix by Steve Blackman and developed by Jeremy Slater. It revolves around a dysfunctional family of adopted sibling superheroes who reunite to solve the mystery of their father's death and the threat of an imminent apocalypse. Season 3 of this loved web series just released over the OTT platform.
Masoom on Disney+ Hotstar
The latest web series, Masoom, started streaming on Disney+ Hotstar on 17th June. The series is based on a twisted family secret that stems from the death of Balwant Kapoor (Upasana Singh), wife of Dr. Balraj Kapoor (Boman Irani). The show goes through unfolding the mysteries and circumstances surrounding her death.
Money Heist: Korea – Joint Economic Area on Netflix
Money heist fans can look forward to something. A new show called Money Heist: Korea – Joint Economic Area is a South Korean television series based on the Spanish heist crime drama series of the same name. The Korean series directed by Kim Hong-sun and written by Ryu Yong-jae is an original Netflix series, starring Yoo Ji-tae, Park Hae-soo, Jeon Jong-seo, Lee Won-jong, and Park Myung-hoon. Set in the same fictional universe as the original series, it depicts a hostage crisis situation set in the Korean Peninsula, involving a genius strategist and people with different personalities and abilities. It was released on June 24, 2022, on Netflix.
That's it for this weekend. You can keep a check on our blog each week to stay updated with the latest weekend series to binge-watch.
Tags: 'The Umbrella Academy', Amazon prime, Content Creator, Disney, Hotstar, instagram, masoom, Money Heist, moneyheist, Netflix, Netflix India, netflix originals, OTT, reels, sonyliv, trending, YouTube
She enjoys reading but is slow at it, loves making people laugh but cracks PJs occasionally, and is excessively communicative most of the time. Veera accepts people as they're while judging them on their face.
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The Steinway Society celebrates its eighteenth season. Over the past eighteen years we have presented outstanding pianists in more than 100 concerts and musicales.
A native of China, Shan-shan Sun was admitted to the Young Artist Program at the Shanghai Conservatory of Music at the age of nine. The following year, she was invited to perform for Mr. Jiang, president of China. Ms. Sun has an active international career that finds her performing throughout the United States, Europe and Asia. The Miami Herald noted that her "intensity brought to mind Alicia de Larrocha's visionary Mozart interpretations." Ms. Sun has recently appeared with Sweden's Gothenburg Symphony Orchestra and the Warmland Sinfonietta, the Liepaja Symphony Orchestra in Latvia, the Amalfi Coast Festival Orchestra in Italy and the Canton Symphony in Ohio. Shan-shan Sun has recorded 4 compact discs, released by China Records, and Mindfeel Records in Sweden. Ms. Sun has won prizes in the Darius Milhaud Competition, the Nina Wideman Piano Competition and the South Orange Symphony Artist Competition. In December 2003, she and her piano duo partner, Per Tegstrand took First Prize at the prestigious Murray Dranoff International Two Piano Competition in Miami, Florida. Today's program will include works by Chopin and Ravel.
L. Scott Donald is the Administrative Director and member of the Senior Faculty at the New School of Music in Kingston, NJ. At The College of New Jersey, as adjunct faculty member, he teaches class piano for music majors. Dr. Donald's performances span the music of Mozart through Gershwin and Brahms through Bernstein. His research involves studying the motor skill development in piano performance and the structure of practice. Dr. Donald studied piano with John Roberts at Furman University and Danielle Martin at the University of Texas where he also studied pedagogy with Robert Duke, Martha Hilley, and Amanda Vick Lethco. He earned his D.M.A. at the University of Texas at Austin. He is a member of Music Teachers National Association, New Jersey Music Teachers Association, National Guild of Community Schools for the Arts and a member of the research committee for the National Conference on Keyboard Pedagogy. Today's performance will feature works by Bach, Beethoven, Brahms and Barber.
Ms. Tao has won enthusiastic audience reception and critical acclaim across the United States and Europe. Born in Miami, Florida, she began her piano studies at the age of five and performed as soloist with orchestra at age ten. The following year, she was a soloist with Arthur Fiedler. Distinguished awards were bestowed to Ms.Tao by the Maryland International Competition, the NY Young Artists in Recital, and the Baldwin National Piano Competition. Selected as Musical Ambassador by the United States Information Agency, she toured throughout Europe giving numerous recitals and master classes. As soloist, Ms. Tao has performed in Carnegie/Weill Recital Hall, Merkin Hall, and the halls of The New York Historical Society and the New School. Overseas, her talent has been heard in the Philharmonic Hall in Lublin, Poland, The Chopin Music Academy in Warsaw, Poland, the Liceo Music Conservatory in Barcelona, Spain and the Esplanade Theatre in Singapore. Ms. Tao has recorded for Centaur Records and Eroica Records. Her performance will include works by Schubert, Medtner and Chopin.
Dr Joanna Chao, Taiwanese pianist, concertizes throughout the United States and abroad. New York Metropolitan audiences have heard her concerts at Carnegie-Weill Recital Hall and Merkin Concert Hall. She has performed as guest soloist with the Moscow Philharmonic Orchestra, Fremont-Philharmonic and New Britain Symphony Orchestra to critical acclaim describing her ability as a "stunning exhibition of virtuosity and style…, with elegance and pure lyrical expression." Dr. Chao has been awarded prize recognition at the Puigcerda International Piano Competition, Bergen Philharmonic Young Artist Competition, The Kingsville International Young Performer's Competition, and the Kosciuzco Foundation Chopin Piano Competition. Dr. Chao has performed for the New York Philharmonic Chamber Ensemble Series, the Sarasota Music Festival, Manchester Music Festival and is a member of the Argento Chamber Ensemble. Dr. Chao studied at the Juilliard School and the Peabody Institute of John Hopkins University with Oxana Yablonskaya and Ellen Mack. She currently serves on the piano faculty at The College of New Jersey and ear-training faculty at The Juilliard School Pre-College Division. Today's program will include compositions by Bach-Busoni, Beethoven, Smetana, Messiaen and Chopin.
Acclaimed by the Moscow News as "a forceful mature personality with a phenomenal technique and playing of emotional depth," Alex Ruvinstein began his music studies at the age of five. He received his Bachelor's degree from the Uman State College and his Master's degree at the Gnesin Academy in Moscow. After receiving his Doctorate at the Maimonides State Academy in Russia, Mr. Ruvinstein served as Professor of Piano at this institution from 1995 to 2006. Playing piano four hands with Olga Gurevich, the duo won the XXVII International Competition in Salerna, Italy and received the top prize in their division at the Ibla International Piano Competition. His solo and chamber music performances included a recital at Weill Recital Hall at Carnegie Hall, participating in New York Library Concert Series, as well as concerts at the United Nations Concert Hall. Currently, Mr. Ruvinstein is principal accompanist at "Hands On", A Musical Experience, Inc. in New York City. His program will include compositions by Bach, Chopin and Ravel.
Karen Walwyn, successfully made her New York debut at Merkin Hall, followed by her debut performance on National Public Radio (NPR). Her most noted performances included works from her compact discs entitled Dark Fires: 20th Century Music for Piano, Vol.I and Dark Fires: Walwyn and Friends, Vol. II (Albany Records). Ms.Walwyn has been in high demand across the United States and in Europe. Following her performance at the Cleveland Museum of Art, the Cleveland Plain Dealer reported: "Walwyn was fearless throughout managing every challenge with precise fingers and heroic command of textures." She serves on the faculty of Howard University in Washington, D.C. as professor of piano. In response to the events of September 11, 2001, Ms. Walwyn composed "Reflections on 9/11". The premiere performance received a standing ovation and a CD will be released shortly by Albany Records. Today's program will include selections from "Reflections on 9/11" along with compositions by Amy Beach, Clara Schumann and Fanny Mendelssohn.


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The Ashtamangala Prasnam revealed that the benevolent Goddess Annapoornesvari, one of the three deities of Srithrukkulasekharapuram temple at Annakara is the 'Dharmadaivam' of the Ullanat family. There was a Vishnu temple in a place called Kokkur and when this temple was destroyed, probably during the invasion of Tippu Sultan, the idol of the Lord was carried and brought by the then Karanavar of Ullanat Tharavad and installed in this temple complex. The Ashtamangala Prasnam revealed that this Lord, known as Kokkur Srikrishnan is also very special to the Ullanat family.Originally this temple of Goddess Annapoornesvari at Annakara was under the control of Ullanat family, but now it is a temple under the management of Hindu Religious & Endowment Council (Malabar), Kozhikode.
There was a huge banyan tree said to be more than 300 years old in front of this temple and the base platform, constructed in red stone, had the name of Ullanat Kunjayamma (40) – mother of Raman Mootha Panicker, being the one . who donated for the construction. A few years ago this tree fell down and the base has also been removed. The entrance gate and a portion of the temple were recently renovated by Mr.P.B.Menon, son of Raghava Panicker (71).


text:
Q: ERROR: cannot be cast to androidx.navigation.fragment.NavHostFragment. -- app crashing every time So I'm trying to build an app with a bottom navigation bar that will switch between fragments.
I did the coding according to some documentation.
I tried every solution on the internet but none of them seems to work for me.
the error:
Caused by: java.lang.ClassCastException: com.example.jetpacklesson.MainFragment cannot be cast to androidx.navigation.fragment.NavHostFragment
        at com.example.jetpacklesson.MainActivity.onCreate(MainActivity.java:30)

here is the XML main activity code
<androidx.constraintlayout.widget.ConstraintLayout xmlns:android="http://schemas.android.com/apk/res/android"
    xmlns:app="http://schemas.android.com/apk/res-auto"
    xmlns:tools="http://schemas.android.com/tools"
    android:layout_width="match_parent"
    android:layout_height="match_parent"
    tools:context=".MainActivity">

    <androidx.fragment.app.FragmentContainerView
        android:id="@+id/firstFragmentHolder"
        android:layout_width="0dp"
        android:layout_height="0dp"
        android:name="com.example.jetpacklesson.MainFragment"
        app:defaultNavHost = "true"
        app:layout_constraintBottom_toTopOf="@+id/bnv_bottomBar"
        app:layout_constraintEnd_toEndOf="parent"
        app:layout_constraintStart_toStartOf="parent"
        app:layout_constraintTop_toTopOf="parent"
        app:navGraph = "@navigation/nav_graph"/>

    <com.google.android.material.bottomnavigation.BottomNavigationView
        android:id="@+id/bnv_bottomBar"
        android:layout_width="0dp"
        android:layout_height="wrap_content"
        app:layout_constraintBottom_toBottomOf="parent"
        app:layout_constraintEnd_toEndOf="parent"
        app:layout_constraintStart_toStartOf="parent"
        app:menu="@menu/nav_bottom_navigation" />
</androidx.constraintlayout.widget.ConstraintLayout>

and main activity java code:

    BottomNavigationView bnv_navigationBar;

    @Override
    protected void onCreate(Bundle savedInstanceState) {
        super.onCreate(savedInstanceState);
        setContentView(R.layout.activity_main);

        NavHostFragment navHostFragment = (NavHostFragment) getSupportFragmentManager().findFragmentById(R.id.firstFragmentHolder);
        NavController navController = navHostFragment.getNavController();
        bnv_navigationBar = findViewById(R.id.bnv_bottomBar);
        NavigationUI.setupWithNavController(bnv_navigationBar, navController);
    }

A: Your XML file says:
android:name="com.example.jetpacklesson.MainFragment"

If you want that to be a NavHostFragment, you need to change that to
android:name="androidx.navigation.fragment.NavHostFragment"

As per the Navigation Getting Started guide.

redpajama_set_name: RedPajamaStackExchange


We have had a fantastic two week trek to . Our Guide and porter. Sanjib and Pemba have been excellent and very attentive looking after us.Sanjib is a very good guide and taught us allot about Nepali culture. Pemba was a brilliant porter. We think he will make an excellent guide in future.The level of service from both Sanjib and Pemba was superb. They were available all the way to help us with anything we needed, and both were thoughtful about anything we might require, water, food showers,accommodation. Sanjib's knowledge of the area and the lodges meant that we were always happy with our accommodation. He took care to visit places which were comfortable and had homestay feel. Sanjib have the qualities to be excellent guide and porter and to give all his clients a wonderful trekking experience.We highly recommend him.
I just wrote a recommendation about this Independent trekking Mr Sanjib which was the one I chose to do Everest Base Camp and Gokyo, I went to Nepal in Feb-March 2015 and I would totally recommend them. Check it out and read below what i also wrote about them. Enjoy yur time in Nepal 🙂 http://www.nepalguideinfo.com sanjib-adhikari@hotmail.com I did Everest Base camp and Gokyo with the Independent trekking guide Mr. Sanjib and after such a nice trek I can only recommend the service that Sanjib and his team provided it. experienced guide, a clear itinerary with lots of room for your own personal pace, a personalized approach: you go to him as a client and you leave as a friend. All this and more make the service of this trek, out of the rest. Prices are very good and the quality of all the services, were excellent. We got only great rooms and they always make sure, we have a nice view from our room (probably this is not always possible, but I like that Sanjib and Raj. were taking time in such a details to make his clients happy) He also advise you in all the matters of the trek and more importantly he was very clear about what you get. Many companies will promise you all kind of things even if they know is not possible (flying to Lukla for example is one of them or how many days you can reach certain altitude being safe from AMS) There's a lot of companies in Kathmandu and I know how difficult and overwhelming the search for the right one can be, but if you're reading this and looking for a person who can make your treks in Nepal smooth and a very enjoyable experience… go to Sanjib and he'll handle the rest ☺ Thanks a lot Sanjib, for organizing my trek in Nepal and if I come back someday I definitely know where to go for treks!!


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text:
Home Vancouver Was Awesome Series Vancouver Was Awesome: A Temple for Labour
Vancouver Was Awesome Series
Vancouver Was Awesome: A Temple for Labour
Lani Russwurm
A Vancouver time travelogue brought to you by Past Tense.
Entrance to the Labor Temple, 411 Dunsmuir Street. Photo by Lani Russwurm
While the destruction of old buildings gets most of the attention in Vancouver these days, it's good to sometimes stop and notice the ones that survive and the stories they tell. The recently renovated Labor Temple at 411 Dunsmuir Street is one splendid old building with a dramatic history.
Designed by architect Thomas Hooper, the building opened in the spring of 1913 at a cost of about a hundred and fifty thousand dollars. It included meeting halls, a large billiards room in the basement, a lounge for unemployed workers, a print shop, a cooperative store to provide low cost goods to workers, and offices for the Vancouver Trades and Labour Council (VTLC), the Socialist Party, and individual unions. It was designed so that a couple more floors could be added in case the need arose.
The Labor Temple was a stop for many prominent and sometimes notorious union leaders passing through town. Mother Jones, IWW co-founder Big Bill Haywood, and Lucy Parsons, the outspoken widow of Haymarket Riot martyr Albert Parsons, are perhaps the most well-known. But it wasn't just radicals who made use of the Labour Temple; the conservative Vancouver Police Union also got its start there when it became one of the first police unions in the country in 1918.
Architect's drawing of the Labor Temple. Vancouver Daily World, 11 March 1911
Canada's first General Strike broke out Vancouver in 1918 following the police killing of union organizer Ginger Goodwin. As part of their strikebreaking effort, employers sent a mob of soldiers to the Temple to intimidate and harass union organizers. The soldiers trashed the place, threw documents out the window and attempted to do the same with two union leaders.
During another general strike in 1919, tensions were heightened by the placement of machine guns atop the Beatty Street Drill Hall a few blocks to the east, which strike supporters complained were aimed at the Labor Temple to intimidate strikers. (More realistically, the guns were well within range of the Cambie Street Grounds, a popular site for rallies across the street).
Mob attacking the Labor Temple during a one day general strike in 1918. "Scene of the clash," Vancouver Daily World, 3 August 1918
Ultimately the Temple became a casualty of this militant period in Vancouver's labour history. A factional split in the VTLC paralyzed its ability to meet the financial obligations of the Labor Temple. The provincial government purchased the building and repurposed it as the first home of Van Tech high school in 1921.
The province retained ownership until a few years ago when it sold the Temple to the current owners. Labour's Vancouver temple is now the Maritime Labour Centre on Victoria Drive, an unsightly but functional headquarters for the Vancouver District Labour Council (the VTLC's current name) that features a fabulous 1940s mural by Fraser Wilson
A longer version of this post can found here.
Dunsmuir Street
Labor Temple
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